THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS
THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS
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DOI：
10.1088/0004-637x/771/2/129
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发表时间：
2013-05
期刊：
影响因子：
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通讯作者：
S. Andrews;K. Rosenfeld;A. Kraus;D. Wilner
中科院分区：
文献类型：
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作者：
S. Andrews;K. Rosenfeld;A. Kraus;D. Wilner
我们基于亚毫米阵列的新“快照”λ = 1.3 mm 巡天，对金牛座恒星形成区域的星周尘埃盘的毫米波连续光度测定目录进行了大幅扩展。将这些新数据与文献中的测量结果相结合，我们构建了 II 类盘的毫米波光度分布 f(Lmm)，对于光谱类型早于 M8.5 的恒星宿主来说，该分布在统计上是完整的，并且 3σ 深度约为 3 mJy。由此产生的普查消除了长期以来针对晚型宿主盘的选择偏差，从而证明 Lmm 和宿主光谱类型之间存在很强的相关性。通过将赫兹普龙-罗素图中单个恒星的位置转化为质量和年龄，并采用 Lmm 和盘质量 Md 之间的简单转换，我们确认这种相关性对应于尘埃盘质量和承载它们的恒星之间统计上稳健的关系。贝叶斯回归技术用于在存在测量误差、数据审查和显着的固有散射的情况下表征这些关系：最佳拟合结果表明，1 M☉ 主机的典型 1.3 mm 通量密度为 ∼25 mJy 和幂律缩放。我们建议，在从 Lmm 到 Md 的转换过程中对尘埃温度进行合理的处理有利于固有的线性 Md∝M* 缩放，典型的盘与星质量比为 ∼0.2%–0.6%。围绕该回归曲线测得的均方根离散度为±0.7 dex，这表明这些盘中不同进化状态、尘埃不透明度和温度的综合影响在任何给定宿主质量下的推断Md（或Lmm）上留下了大约40倍的半最大范围全宽。我们认为，Md 和 M* 之间的这种关系可能代表了系外行星群中巨行星频率与主恒星质量之间推断相关性的起源，并为行星形成的核心吸积模型提供了一些基本支持。此外，我们警告说，在圆盘演化的比较研究中必须考虑不完整性和选择偏差的影响，并通过此处介绍的金牛座目录与蛇夫座、IC 348 和上斯科年轻星团中的不完整子样本之间的 f(Lmm) 统计比较来说明这一事实。
We present a substantial extension of the millimeter (mm) wave continuum photometry catalog for circumstellar dust disks in the Taurus star-forming region, based on a new “snapshot” λ = 1.3 mm survey with the Submillimeter Array. Combining these new data with measurements in the literature, we construct a mm-wave luminosity distribution, f(Lmm), for Class II disks that is statistically complete for stellar hosts with spectral types earlier than M8.5 and has a 3σ depth of roughly 3 mJy. The resulting census eliminates a longstanding selection bias against disks with late-type hosts, and thereby demonstrates that there is a strong correlation between Lmm and the host spectral type. By translating the locations of individual stars in the Hertzsprung–Russell diagram into masses and ages, and adopting a simple conversion between Lmm and the disk mass, Md, we confirm that this correlation corresponds to a statistically robust relationship between the masses of dust disks and the stars that host them. A Bayesian regression technique is used to characterize these relationships in the presence of measurement errors, data censoring, and significant intrinsic scatter: the best-fit results indicate a typical 1.3 mm flux density of ∼25 mJy for 1 M☉ hosts and a power-law scaling . We suggest that a reasonable treatment of dust temperature in the conversion from Lmm to Md favors an inherently linear Md∝M* scaling, with a typical disk-to-star mass ratio of ∼0.2%–0.6%. The measured rms dispersion around this regression curve is ±0.7 dex, suggesting that the combined effects of diverse evolutionary states, dust opacities, and temperatures in these disks imprint a full width at half-maximum range of a factor of ∼40 on the inferred Md (or Lmm) at any given host mass. We argue that this relationship between Md and M* likely represents the origin of the inferred correlation between giant planet frequency and host star mass in the exoplanet population, and provides some basic support for the core accretion model for planet formation. Moreover, we caution that the effects of incompleteness and selection bias must be considered in comparative studies of disk evolution, and illustrate that fact with statistical comparisons of f(Lmm) between the Taurus catalog presented here and incomplete subsamples in the Ophiuchus, IC 348, and Upper Sco young clusters.